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NCAR/TN-213+STR NCAR TECHNICAL NOTE _ I I I -I 1~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~ July 1983 The Second Joint Solar Dynamics Project Data Summary Solar Magnetic Field, Chromospheric and Coronal Observations Near the Time of the 11 June 1983 Solar Eclipse D.G. Sime, R.R. Fisher, C.J. Garcia, J.R. Najita, K.A. Rock, P.H. Seagraves, and E.A. Yasukawa, NCAR M.K. McCabe and D.L. Mickey, University of Hawaii HIGH ALTITUDE OBSERVATORY I ~~~~~~-- NATIONAL CENTER FOR ATMOSPHERIC RESEARCH BOULDER, COLORADO iii CONTENTS page PREFACE v. I. INTRODUCTION . 1 II. MLSO DATA PRODUCTS 4 III. MSO DATA PRODUCTS 8 IV. DATA COVERAGE 11 V. SOLAR ACTIVITY DURING THE SOLDYN II PERIOD 13 VI. DAILY SOLAR DATA 17 VII. SYNOPTIC SOLAR DATA 51 ACKNOWLEDGMENTS 57 REFERENCES 59 V PREFACE The success of the first Joint Solar Dynamics Project (SOLDYN I) observing period (see NCAR Technical Note TN-202+STR and Fisher et al., 1983) demon- strated the power of the integrated operation and co-ordination of instruments available in the Hawaiian islands in producing a wide-ranging observational record of conditions on the sun. Examination and analysis of the data collected made it clear that this instrumentation would also allow the collection of a valu- able record of the sun near the time of the 11 June 1983 solar eclipse. Such a record would be valuable to the High Altitude Observatory (HAO) and University of Hawaii (U of H) eclipse expedition scientific analysis efforts, and would also provide a valuable context for the community at large in which to interpret its own eclipse observations. Further, the observations would give an opportunity to verify whether the observed relationships established during SOLDYN I were maintained on the sun a year later in the solar cycle. At a planning meeting which took place on 18 April 1983, during the 3rd Hawaiian Neighborhood Meeting in Honolulu, the decision was made to carry out these co-ordinated observations under the name SOLDYN 11. This Technical Note presents the observations made during this effort in the interval 3-17 June 1983. As far as possible, daily observations made with the Mark-Ill k- coronameter of the Mauna Loa Solar Observatory (MLSO) as well as photo- graphic records of the sun in Ca II and Ha, and from the flare patrol at Mees Solar Observatory (MSO) on Haleakala, Maui, are included. We also present daily observations of the longitudinal component of the photospheric magnetic field made at MSO. Finally, the coronal and magnetic field observations are assem- bled into synoptic maps for the period near the eclipse. D. G. Sime, July 1983 High Altitude Observatory I. INTRODUCTION The general goal of the HAO/University of Hawaii Joint Solar Dynamics Pro- ject is to establish the relationships that exist between the solar magnetic field as detected in the photosphere and the structure and evolution of the corona. The SOLDYN program of 19B2 (see Fisher et al., 19B2a) demonstrated our ability to use existing instruments to gather data of value in the pursuit of that goal. During that program, which ran from 14 June to 13 August 1983, daily co- ordinated observations were made of the sun and corona using the Mark-111 k- coronameter and the prominence monitor at HAO's Mauna Loa Solar Observa- tory (MLSO) and the Stokes polarimeter, Ha flare patrol and Ca II cameras, and the Ha coronagraph at U of H's Mees Solar Observatory (MSO). This wide rang- ing record of the sun enabled us to begin to address specific questions in par- tial satisfaction of our goal (Fisher et al., 1983) and encouraged us to believe that additional observations in the summer of 1983 would be of value. Specifi- cally, these new data would allow us to achieve three ends: (1) Document the state of the sun, from the photosphere up through the chro- mosphere and out into the corona for the two week period around the total solar eclipse of 11 June 1983, (2) Specify the relationship between the photospheric magnetic fields and the temperature and density structure of the corona, and (3) Verify the relationship between inferred coronal mass and the observed Ca II K-line plage area which was established during the SOLDYN project. In this NCAR Technical Note, we present the reduced observations made during the SOLDYN II period and necessary to achieve these goals. They are presented both in the form of daily photographic and photo-electric measure- ments, and in synoptic format for the period. 2 To satisfy the scientific requirements of the program, the following comrple- ment of observations was defined for each day: Mees Solar Observatory (MSO): (1) One Stokes polarimeter scan of the center third of the disk at XG3Jo3 (2) One Ca 11 K-line, 0.3A FWHM filtergram of the full disk (3) One Ha, 0.5A FWHM, on-band filtergram of the full disk (4) One Ha, 0.5A FWHM, off-band filtergram of the full disk, AkX-A1 (5) One Ha, t 7.6A FWHM, full-limb image Mauna Loa Solar Observatory (MLSO): (1) One contour plot of the inner coronal pB distribution as a function of posi- tion angle and height from 1.3 to 2.1 Jo (2) Two plots of inferred pB as a function of latitude and longitude, called SHELL, for heights above the limb of 1.3 fP and 1.7 /Ki (3) One daily DIMAGE difference image plot, a subtraction of the previous day's synoptic pB image from the present day's data. (4) One Ha, 0.5X FWHM, disk image (back-up only). (5) One Ha, B.1A FWHM, full-limb image (back-up only). In addition to the daily central disk scans with the Stokes polarimeter, on the 10th and 12th of June, extra scans, encompassing the West (on the 10th) and the East (on the 12th) limbs, were made.: In spite of the varied and changeable observing conditions, the skill and perseverance of the two observatory site crews paid off in an almost complete set of observations. The full basic daily set of data was achieved on 1.4 out of 15 days; a tribute to the effectiveness of both individual and team efforts. Both 3 sites were active on 100% of SOLDYN II observing days as shown in Table 2. The sky was generally clearer for these observations than it was last summer, and the weather was generally fair, providing favorable observing conditions on the whole, particularly in the mornings. The sun was not particularly active during these observations, and the active regions which we observed were quite well spread out over the entire sun, in contrast to last year's conditions. No coronal transients were observed either during Mark-111 operations or by deduction from the daily DlVIAGE. On the final day of operations for SOLDYN II, a large EPL event occurred on the Southeast limb, but no observed coronal transient was associated with it. The limb at eclipse time seemed rather quiet. The activity noted by the observers is summarized in Table 3. 4 II. MLSO DATA PRODUCTS The observations carried out at MLSO provided 2 data sets; photo-electric measurements of the polarized coronal radiance, and photographic records of the limb and disk of the sun. Mark-Ill The Mark-ll k-coronameter is a 23 cm diameter objective iadging k- coronameter, which produces digital images at the rate of three images every 184 s. This system has been described by Fisher et al. (1961), and is the major piece of instrumentation at MLSO. Digital images are recorded onto 1,600 bpi nine-track magnetic tape. During the SOLDYN II period, three types of reduced data were produced. These were: (1) A calibrated contour plot of the coronal pB distribution (1MAP) (2) Two inferred coronal pB distributions plotted onto spherical projections, one each for heights of 1.3 Jo and 1.7 fJo (SHELL) (3) Contour plots of the daily one-day difference pB distribution (DIMAGE). For more discussion of these data products, the reader is directed to the dis- cussion by Rock and Seagraves (1982); some more detail is given below. P-MON The prominence monitor at MLSO is an internally occulted telescope which is used to observe the sun's limb, and which provided the photographic data from MLSO. A solar image, 11.5-mm in diameter, is recorded on 35-mm SO-2415 film giving a plate scale of 166.9 arc seconds/mm. The Ha disk is observed by using a Ak FWHM X6563 filter. The observing format used is a three frame graded sequence of an under-, nominal- and over-exposed image of the limb through an B.1A FWHM interference filter usually followed by a single disk image. Several pauses are programmed into the routine to allow the observer to view the sun with the television camera for activity awareness. One loop of the film sequence requires 4 min to complete. This monitoring program was run continuously from about 1 h after dawn until shutdown at approximately local noon. The MLSO crew was able to operate the prominence monitor 14 days out of the 15 days of the solar dynamics observing program. 1MAP The 1MAP program became part of the MLSO observing procedure on 31 January 1982. It replaces all previous coronal mapping programs for the daily data archive. The map is proportioned to agree with the instrument's actual field of view, which extends roughly between 1.2 and 2.1 fiP. To give an irnmmedi- ate idea of the coronal pB amplitude, there is a single polar plot of pB in the center of the graph, which is taken at the height of 1.35 Ro.

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